[IAUC] CBET 1898: 20090806 : V582 AURIGAE

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                                                  Electronic Telegram No. 1898
Central Bureau for Astronomical Telegrams
INTERNATIONAL ASTRONOMICAL UNION
M.S. 18, Smithsonian Astrophysical Observatory, Cambridge, MA 02138, U.S.A.
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V582 AURIGAE
     U. Munari, A. Siviero, P. Ochner, and M. Fiorucci, Istituto Nazionale di
Astrofisica, Padova Astronomical Observatory; and S. Dallaporta, "Asiago Novae
and Symbiotic Stars" (ANS) collaboration, report that CCD photometry of V582
Aur (cf. CBET 1896) was obtained on Aug. 5.09 and 6.08 UT, yielding magnitudes
B = 17.0 and 16.9, V = 14.78 and 14.83, R_c = 13.49 and 13.50, and I_c = 12.23
and 12.22, respectively.  The calibration was carried out with respect to
local Tycho-2 and 2MASS catalogue stars, using the transformations of Bessell
(2000, PASP 112, 961) and Caldwell et al. (1993, SAAO Circ. 15, 1).  A few
photographic plates imaging the sky position of V582 Aur have been located in
the archives of the Asiago Schmidt telescopes; V582 Aur appeared below the
plate limits, which were mag B = 16.0 on 1975 May 2, and V = 14.8 and B = 16.0
on 1980 Feb. 14.  A low-resolution CCD spectrum (0.24 nm/pixel; range 380-700
nm) was obtained on Aug. 6.12 with the 1.22-m telescope of the Asiago
Astrophysical Observatory, attaining S/N = 50 around H_alpha.  The spectrum is
dominated by absorption lines of the Balmer series (the equivalent width of
H_alpha was 0.52 nm), Na I D (EW = 0.43 nm) and Ba II 649.6-nm (EW = 0.20 nm).
No emission line is evident on the spectrum, whose overall appearance is that
of a super giant of temperature about 5500 K, and pretty close to that of
V733 Cep (an object of the FU Ori type) as presented by Reipurth et al.
(2007, A.J. 133, 1000).  A significant difference is the Li 670.7-nm line,
which is strong in V733 Cep and weak in the spectrum of V582 Aur, not
emerging above the noise.


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                         (C) Copyright 2009 CBAT
2009 August 6                    (CBET 1898)              Daniel W. E. Green